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arxiv: 2606.27057 · v1 · pith:Y7CQTSTTnew · submitted 2026-06-25 · 🌌 astro-ph.GA

Unveiling a cosmic tango: Integral field spectroscopy and numerical simulations of Arp 143's interaction

Hugo Martel , Carmelle Robert , Laurent Drissen , Charles-Antoine Parent , Prime Karera , S\'ebastien Vicens-Mouret , Salvador Duarte Puertas , Jorge Iglesias P\'aramo
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Jos\'e M. Vilchez
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Pith reviewed 2026-06-26 03:34 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords Arp 143ring galaxygalaxy interactionintegral field spectroscopychemodynamical simulationtidal plumeNGC 2445star formation
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The pith

Simulations indicate Arp 143 formed from a head-on collision between an S0 and Sc galaxy after a flyby encounter.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

This paper presents integral field spectroscopy of Arp 143 that maps gas kinematics and oxygen abundances across the ring galaxy NGC 2445 and its companion NGC 2444. It combines these maps with chemodynamical simulations to reconstruct the galaxies' interaction history. The observations show an expanding ring with non-circular flows, an off-center nucleus, and slightly sub-solar abundances in the ring. The models reproduce the data only for a sequence that begins with a flyby creating the long plume from disk debris followed by a head-on collision. A reader would care because this pins down the specific geometry that turns two galaxies into a ring plus plume system with localized star formation.

Core claim

Spectral data cubes reveal strong non-circular flows in the expanding ring of NGC 2445, an off-centered nucleus, and oxygen abundances that are on average slightly sub-solar in the ring but near solar in the nucleus. The long tidal plume has a faint stellar counterpart visible in broad-band images. Chemodynamical simulations of the system match the observed kinematics, morphology, and chemical properties when the encounter starts with a flyby between the disk galaxy and the S0 that strips material into the plume, followed by a head-on collision that forms the ring.

What carries the argument

The chemodynamical evolution code that tests interaction histories and reproduces the observed kinematics, morphology, and chemical properties only under the head-on collision after flyby scenario.

If this is right

  • The ring in NGC 2445 formed from the head-on collision phase.
  • The long plume consists of debris stripped from the disk galaxy during the earlier flyby.
  • Star-forming regions remain concentrated in the ring and nucleus because the interaction compresses gas there.
  • The nucleus sits off-center relative to the ring as a direct result of the collision dynamics.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • Similar chemodynamical modeling applied to other collisional ring galaxies could test whether head-on collisions after flybys are a common formation channel.
  • The requirement for a preceding flyby implies that many ring systems may carry signatures of multi-stage encounters rather than single impacts.
  • The measured abundance contrast between ring and nucleus could be used to time how quickly newly formed stars enrich the gas during the encounter.

Load-bearing premise

The chemodynamical simulations reproduce the observed kinematics, morphology, and chemical properties only under the specific head-on collision plus flyby scenario, and alternative interaction histories would not match the data equally well.

What would settle it

A simulation of an alternative interaction geometry or sequence, such as a non-head-on impact without a prior flyby, that matches the velocity maps, abundances, plume structure, and star-formation locations equally well would falsify the uniqueness of the proposed history.

Figures

Figures reproduced from arXiv: 2606.27057 by Carmelle Robert, Charles-Antoine Parent, Hugo Martel, Jorge Iglesias P\'aramo, Jos\'e M. Vilchez, Laurent Drissen, Prime Karera, Salvador Duarte Puertas, S\'ebastien Vicens-Mouret.

Figure 1
Figure 1. Figure 1: Composite coloured image of the central part of Arp 143 obtained with SITELLE (blue: SN2 deep image, red: SN3 deep image enhanced with the pure H𝛼 emission flux map, green: mean of SN2 and SN3 deep images). The image spans 3 ′ × 3.6 ′ , which is about 10% of the total SITELLE FOV. North is up and East is left [PITH_FULL_IMAGE:figures/full_fig_p002_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Emission lines flux maps of NGC 2445 extracted from the data cubes. The FOV is 1.6 ′ × 1.6 ′ , with North at the top and East to the left. 2.2 Dragonfly The Dragonfly Telephoto array is a robotic telescope array that consists of 48 Canon 400 mm 𝑓 /2.8 IS II lenses with special anti￾reflective coatings on optical surfaces designed to reach surface brightness levels below ∼ 28–29 mag arcsec−2 (Abraham & van … view at source ↗
Figure 3
Figure 3. Figure 3: Hii region complexes domain (black contours) identified by the detection code overlaid on the Hα amplitude map of NGC 2445. 1 2 3 4 Hα FeI Hβ Data PPXF abs. fit H10 H14 14800 15000 15200 15400 15600 0 1 Flux 10 −15 erg/s/cm 2 /˚A 20000 20500 21000 Wavenumber [cm−1 ] Data – PPXF abs. fit 26500 27000 27500 800 1000 1200 X 800 1000 1200 Y Deepframe SN3 [PITH_FULL_IMAGE:figures/full_fig_p004_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Left: PPXF absorption model for the global stellar population of the ring galaxy. In black, the integrated spectrum of ∼ 5200 pixels with a continuum SNR above 7 and an Hα emission flux below 1 × 10−19 erg cm−2 s −1 , fter being set to the restframe velocity using our rotation model. In red and blue, the PPXF absorption fit and residual, respectively. Right: selected pixels for the stellar population model… view at source ↗
Figure 5
Figure 5. Figure 5: Comparison of the Hα and Hβ flux of the emission regions for the observed values (red), with the stellar population correction (blue) and when a 3Å EQW is simply added. Only regions with an SNR > 3 for both lines are considered. Median values for the 3 distributions are given on the plots. the ring galaxy, we also masked the companion galaxy. Imposing a minimum value of 7 for the continuum SNR and a maximu… view at source ↗
Figure 6
Figure 6. Figure 6: Dust extinction as a function of the galactocentric distance. Only regions with a SNR > 5 in Hα and Hβ are shown. Left: each region is colour-coded by its Hα flux. The dashed line indicate a 0 mag extinction. The black line represents a linear regression done while excluding the nucleus and regions with a negative extinction. The slope of the regression is given on the plot (along with its p-reliability te… view at source ↗
Figure 7
Figure 7. Figure 7: Dust extinction colour-coded by the location angle. Left: as in the previous figure, regions extinction is shown as a function of their GCD, with the linear regression, but here colour-coded with their location angle. As shown on the map to the right, the location angle is set to 0 ◦ on the dynamical axis of NGC 2445 and increases toward the northeast direction (from red-green-blue) considering the inclina… view at source ↗
Figure 8
Figure 8. Figure 8: [Nii] and [Sii]-BTP diagrams colour-coded with the integrated Hα flux of each regions (top), GCD (middle), and location angle (bottom). Only regions (114) with an SNR > 3 for all the lines used here are shown. The emission line fluxes have been corrected for the underlying stellar population but not the extinction (since lines used for a ratio are very close in wavelength). Overlaid are the diagnostic curv… view at source ↗
Figure 9
Figure 9. Figure 9: Maps of emission lines ratios for the emission regions present in the BPT diagrams ( [PITH_FULL_IMAGE:figures/full_fig_p008_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: Oxygen abundances colour-coded with the integrated Hα flux of the regions. The indicators used (see text) are identified on each plot. Only regions with an SNR > 3 for the lines used for an indicator have been considered (the number of regions are given in parenthesis on each plot). The black lines represent the linear regression done while excluding the nucleus; slope are given on each plot (along with t… view at source ↗
Figure 11
Figure 11. Figure 11: Top panel: N2 PP04 oxygen abundances as in [PITH_FULL_IMAGE:figures/full_fig_p010_11.png] view at source ↗
Figure 13
Figure 13. Figure 13: The N/O ratios using equations of P16 (left) and PP04 (right) as a function of the GCD, colour-coded the integrated Hα flux of the regions (top) and the location angle (bottom). 8.0 8.2 8.4 8.6 12+log(O/H) R_P16 1.6 1.4 1.2 1.0 0.8 0.6 0.4 Log(N/O) P16 15.0 14.5 14.0 13.5 L o g ( H Flu x ) [PITH_FULL_IMAGE:figures/full_fig_p011_13.png] view at source ↗
Figure 14
Figure 14. Figure 14: N/O ratio versus metallicity using equations of P16, colour-coded with the integrated Hα flux of the regions. The red dashed line shows the relation of Andrews & Martini (2013) [PITH_FULL_IMAGE:figures/full_fig_p011_14.png] view at source ↗
Figure 15
Figure 15. Figure 15: SN3 spectrum of the nucleus of NGC 2444 (integrated within a radius of 4.5 ′′) [PITH_FULL_IMAGE:figures/full_fig_p011_15.png] view at source ↗
Figure 17
Figure 17. Figure 17: Spectrum of the nucleus of NGC 2445, integrated within a radius of 1.2′′, along with the fit (dashed blue line) [PITH_FULL_IMAGE:figures/full_fig_p012_17.png] view at source ↗
Figure 18
Figure 18. Figure 18: Spectrum of the SE lobe of NGC 2445 (integrated within a radius of 1.2′′), centered on the Hα and [Nii] lines, along with the two-component fit. gion of low ionization, in the shocks region of diagnostic diagrams, and highly turbulent (as suggested by the line widths in the SN3 fil￾ter). Although its nature is unclear, the ionized ridge likely emanates from NGC 2445 from which it has been stripped away du… view at source ↗
Figure 20
Figure 20. Figure 20: Left: Composite coloured image of Arp 143 obtained with Dragonfly Telephoto Array (blue: g band deep image, red: r band deep image, green: mean of g and r deep images). The blue tidal plume is visible. Right: VLA C + D Hi map of the same field (Appleton et al. 1987). The images span 14′ × 17′ . North is up, East is left. The rectangles labeled T1 and T2 denote the location of detected blue star-forming kn… view at source ↗
Figure 21
Figure 21. Figure 21: Left: SITELLE zoomed-in view (1.2 ′ × 2.7 ′ ) of the base of the plume (labeled T1 in [PITH_FULL_IMAGE:figures/full_fig_p014_21.png] view at source ↗
Figure 22
Figure 22. Figure 22: Heliocentric velocity (left) and velocity dispersion (right) of NGC 2445. Contours correspond to a flux of 6 × 10−18erg s−1 cm−2 pixel−1 . FOV is 86′′ on a side, centered at RA 07h46m55.51s, Dec +39°00′49′′ . Since collisional rings are predicted to be expanding caustic waves, a rotation + expansion model is applied to the 2D velocity field of the ring using diskfit. The rotation + expansion model can be … view at source ↗
Figure 23
Figure 23. Figure 23: Hα velocity field (left), best fitted velocity models (middle), residuals (right) to the nucleus (top row) and ring structure (middle row) of NGC 2445. Rotation-only model is applied to the nucleus whereas the ring is fitted with a rotation+expansion model (see text). Radial profiles (bottom row) of the circular and expansion velocities are represented by the continuous (black) and dashed (red) lines resp… view at source ↗
Figure 25
Figure 25. Figure 25: Composite zoom-in surface density map showing, at 𝑡 = 480 Myr, the total stellar surface density (gray scale) and the stellar surface density of young stars, formed during the last 50 Myr (colour scale). The model predicts the presence of young stars in the nucleus of NGC 2445, as well as in the ring, as observed. NGC 2445 in SITELLE data (the observed maximum radial velocity was estimated at a radius of … view at source ↗
Figure 24
Figure 24. Figure 24: Ages of the stars (top) and gas (bottom) at 𝑡 = 480 Myr. For stars, the age is the time elapsed since the star formed. For gas, the age is the time elapsed since the gas was ejected by stellar outflows (winds and SNe). Large values correspond to stars and gas that were present at the beginning of the simulation. ring in Gal2int (and in NGC 2445) is approximately four times bigger and four times faster tha… view at source ↗
Figure 26
Figure 26. Figure 26: Zoom-in view of the gaseous (top left) and stellar (bottom left) surface density maps. For comparison purposes, archival Spitzer and SITELLE composite coloured deep image are presented. In the optical image (bottom right), the morphological structures such as the outer ring, spokes and inner ring in NGC 2445, easily recognizable by their blue colours tracing the young stellar clusters, are well reproduced… view at source ↗
Figure 27
Figure 27. Figure 27: L.o.s. velocity and velocity dispersion of gas in Gal2int, from 40 Myr before to 40 Myr after the present. Each panel is 36 kpc wide. and 40 km s−1 in the disk and nucleus of Gal2iso respectively. High dispersions in Gal2iso are also associated with sites of SF. The expansion of the outer ring is not azimuthally uniform and the shape of the outer ring changes with time. A close look at the snapshots in Fi… view at source ↗
Figure 28
Figure 28. Figure 28: Top panel: temporal evolution of the separation between model interacting galaxies Gal1int and Gal2int. Second panel: evolution of SFR for interacting galaxy Gal2int, within 3 kpc and 10 kpc of the centre. Third panel: evolution of SFR for isolated galaxy Gal2iso. Bottom panel: Ratio of SFRs for galaxies Gal2int and Gal2iso. Vertical dotted lines indicate moments of pericentre passsages; the vertical dash… view at source ↗
Figure 29
Figure 29. Figure 29: Top row : Oxygen abundance maps of the numerical model before the head-on (𝑡 = 420 Myr), right after the head-on collision (𝑡 = 440 Myr), and at best match configuration (𝑡 = 480 Myr). Middle row : Corresponding log(N/O) maps. Bottom row : 12 + log(O/H) and log(N/O) derived from observations. Note the different scale used for log(N/O) maps from the simulations and observations. collision disk that is esse… view at source ↗
Figure 30
Figure 30. Figure 30: Top : Radial profiles of the oxygen abundance in Gal2int (left) and Gal2iso (right) before the outer expanding ring is formed (𝑡 = 420 Myr), right after its formation (𝑡 = 440 Myr), and at best match (𝑡 = 480 Myr). Bottom : Temporal evolution of central (𝑟 < 4 kpc) O, N, and Fe abundances in Gal2int (left) and Gal2iso (right). Vertical lines in bottom left panel have the same meaning as in [PITH_FULL_IMA… view at source ↗
read the original abstract

We present spectral data cubes of the interacting galaxy system Arp 143, composed of the ring galaxy NGC 2445 and the lenticular galaxy NGC 2444, obtained with the imaging Fourier transform spectrometer SITELLE at the Canada-France-Hawaii Telescope. Our data allow to probe the kinematics of the interaction and the chemical properties of the ionized gas. Star-forming regions are almost exclusively found in the ring and nucleus of NGC 2445 with the exception of a few very faint ones discovered at the base of the long tidal plume extending north of NGC 2444. Analysis of the H{\alpha} velocity map reveals strong non-circular flows in the ring of NGC 2445, which is expanding. Its nucleus is off-centered with respect to the ring. Oxygen abundance in the ring is on average slightly sub-solar whereas it is close to solar in the nucleus. Broad-band images obtained with the Dragonfly Telephoto array allow to identify the tenuous stellar counterpart of the radio tidal plume. The interaction between the two galaxies is simulated with a chemodynamical evolution code; these simulations suggest that Arp 143 has resulted from a head-on collision between a S0 and a Sc spiral galaxy following a flyby encounter that triggered the formation of the long plume from debris of the disk galaxy.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 2 minor

Summary. The paper presents integral field spectroscopy of Arp 143 (NGC 2445 ring galaxy and NGC 2444 companion) obtained with SITELLE, analyzing Hα kinematics showing an expanding ring with non-circular flows and off-centered nucleus, plus oxygen abundances that are sub-solar in the ring and near-solar in the nucleus. Broadband Dragonfly imaging reveals the stellar counterpart to the tidal plume, and chemodynamical simulations are used to interpret the system as resulting from a head-on collision between an S0 and Sc galaxy following a flyby encounter that formed the plume from disk debris.

Significance. If the simulations are shown to provide a quantitatively good match, the work supplies a concrete reconstruction of an interaction history that links observed ring expansion, plume morphology, and chemical properties to a specific sequence of encounters. The IFS dataset and identification of faint star-forming regions in the plume are solid observational contributions; the interpretive value depends on demonstrating the robustness of the numerical model.

major comments (2)
  1. [Simulations section] Simulations section: the central interpretive claim rests on the chemodynamical models reproducing the observed kinematics, ring expansion, plume, and abundances under the proposed head-on collision plus flyby scenario. The manuscript must supply the explored parameter ranges (mass ratio, impact parameter, timing), the number of runs performed, and quantitative fit metrics (e.g., residuals to the velocity field or abundance map) so that readers can evaluate whether alternative histories are excluded or merely not tested.
  2. [Kinematics analysis] Kinematics analysis: the statements that the ring is expanding and exhibits strong non-circular flows are load-bearing for the interaction interpretation, yet no numerical values for expansion velocity, residual velocity dispersion after subtracting circular rotation, or comparison to a simple expanding-ring model are provided in the text or figures.
minor comments (2)
  1. The abstract phrasing 'these simulations suggest' is appropriately cautious, but the manuscript should consistently qualify the simulation result as one plausible history rather than the definitive one.
  2. Figure captions for the velocity and abundance maps should explicitly state the spatial resolution, seeing, and any smoothing applied.

Simulated Author's Rebuttal

2 responses · 0 unresolved

Thank you for the detailed and constructive referee report. We address each major comment below and plan to revise the manuscript to incorporate the suggested improvements.

read point-by-point responses

  1. Referee: [Simulations section] Simulations section: the central interpretive claim rests on the chemodynamical models reproducing the observed kinematics, ring expansion, plume, and abundances under the proposed head-on collision plus flyby scenario. The manuscript must supply the explored parameter ranges (mass ratio, impact parameter, timing), the number of runs performed, and quantitative fit metrics (e.g., residuals to the velocity field or abundance map) so that readers can evaluate whether alternative histories are excluded or merely not tested.

    Authors: We agree that the simulations section requires additional documentation to support the central interpretive claims. The revised manuscript will include a dedicated subsection or table specifying the explored ranges of mass ratio, impact parameter, and timing, the total number of runs performed, and quantitative fit metrics (such as velocity field residuals and abundance map comparisons). This will allow readers to better assess the robustness and uniqueness of the proposed scenario. revision: yes

  2. Referee: [Kinematics analysis] Kinematics analysis: the statements that the ring is expanding and exhibits strong non-circular flows are load-bearing for the interaction interpretation, yet no numerical values for expansion velocity, residual velocity dispersion after subtracting circular rotation, or comparison to a simple expanding-ring model are provided in the text or figures.

    Authors: We acknowledge that the kinematics section would be strengthened by quantitative values. In the revision, we will add the measured ring expansion velocity, the residual velocity dispersion after subtracting the circular rotation component, and a direct comparison of the observed velocity field to a simple expanding-ring model, with supporting updates to the text and figures as needed. revision: yes

Circularity Check

0 steps flagged

No significant circularity detected

full rationale

The paper's central claim rests on new integral-field spectroscopy from SITELLE, Dragonfly imaging, and independent chemodynamical simulations that are run to match the observed kinematics, morphology, and abundances. No equations, fitted parameters, or self-citations are presented that reduce the interpretive conclusion to an input by construction. The abstract frames the head-on collision plus flyby scenario as one consistent history suggested by the models rather than a uniqueness theorem or renamed empirical pattern. This is the normal case of an observation-plus-modeling paper whose derivation chain remains externally falsifiable.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 0 invented entities

The claim rests on the validity of the chemodynamical code to model the interaction and the interpretation of the spectral data using standard emission line diagnostics for abundances and velocities.

free parameters (1)
  • chemodynamical simulation parameters (mass ratio, impact parameter, timing)
    The simulations are adjusted to match the observed ring expansion, plume, and abundances, introducing fitted parameters.
axioms (1)
  • domain assumption Standard galactic dynamics and chemical evolution models apply to interpret the velocity fields and oxygen abundances from emission lines.
    Invoked implicitly when analyzing H-alpha kinematics and abundances in the abstract.

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